Astronomy & Astrophysics manuscript no. HD219134˙published © ESO 2019 October 31, 2019 From the stellar properties of HD 219134 to the internal compositions of its transiting exoplanets. R. Ligi1, C. Dorn2, A. Crida3;4, Y. Lebreton5;6, O. Creevey3, F. Borsa1, D. Mourard3, N. Nardetto3, I. Tallon-Bosc7, F. Morand3, E. Poretti1. 1 INAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate, Italy e-mail: [email protected] 2 University of Zurich, Institut of Computational Sciences, University of Zurich, Winterthurerstrasse 190, CH-8057, Zurich, Switzerland 3 Universite´ Coteˆ d’Azur, Observatoire de la Coteˆ d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, CS 34229, 06304 Nice cedex 4, France 4 Institut Universitaire de France, 103 Boulevard Saint-Michel, 75005 Paris, France 5 LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universites,´ UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cite,´ 92195 Meudon Cedex, France 6 Univ. Rennes, CNRS, IPR (Institut de Physique de Rennes) - UMR 6251, F-35000 Rennes, France 7 Univ. Lyon, Univ. Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230 Saint-Genis- Laval, France Received 5 July 2019 / Accepted 20 September 2019 ABSTRACT Context. The harvest of exoplanet discoveries has opened the area of exoplanet characterisation. But this cannot be achieved without a careful analysis of the host star parameters. Aims. The system of HD 219134 hosts two transiting exoplanets and at least two additional non-transiting exoplanets. We revisit the properties of this system using direct measurements of the stellar parameters to investigate the composition of the two transiting exoplanets. Methods. We used the VEGA/CHARA interferometer to measure the angular diameter of HD 219134. We also derived the stellar density from the transits light curves, which finally gives a direct estimate of the mass. This allowed us to infer the mass, radius, and density of the two transiting exoplanets of the system. We then used an inference model to obtain the internal parameters of these two transiting exoplanets. Results. We measure a stellar radius, density, and mass of R? = 0:726 ± 0:014 R , ρ? = 1:82 ± 0:19 ρ , and M? = 0:696 ± 0:078 M , respectively; there is a correlation of 0.46 between R? and M?. This new mass is lower than that derived from the C2kSMO stellar evolutionary model, which provides a mass range of 0.755−0.810 (±0:040) M . Moreover, we find that planet b and c have smaller radii than previously estimated of 1:500 ± 0:057 and 1:415 ± 0:049 R⊕ respectively; this clearly puts these planets out of the gap in the exoplanetary radii distribution and validates their super-Earth nature. Planet b is more massive than planet c, but the former is possibly less dense. We investigate whether this could be caused by partial melting of the mantle and find that tidal heating due to non-zero eccentricity of planet b may be powerful enough. Conclusions. The system of HD 219134 constitutes a very valuable benchmark for both stellar physics and exoplanetary science. The characterisation of the stellar hosts, and in particular the direct determination of the stellar density, radius, and mass, should be more extensively applied to provide accurate exoplanets properties and calibrate stellar models. Key words. Stars: fundamental parameters - Stars:individual: HD 219134 - Planetary systems - Techniques: interferometric - Methods: numerical - Planets and satellites: fundamental parameters 1. Introduction are known. Up to now, most of transiting exoplanet hosts have been very faint, driven by the search for exoplanets rather than their characterisation, often leading to inaccurate and/or impre- arXiv:1909.10058v2 [astro-ph.EP] 30 Oct 2019 The huge harvest of exoplanets discovered by the space tele- scopes Kepler (Borucki et al. 2010) and CoRoT (Baglin 2003) cise stellar parameters. This makes the characterisation of the has led to the understanding that exoplanets are the rule rather whole exoplanetary system difficult and the determination of the than the exception. We have now moved to the era of exo- exoplanetary internal structure approximate. planet characterisation, and the next challenge is to understand Several methods can be employed to obtain the stellar pa- how common rocky planets are and if any are suitable for life. rameters. Concerning the mass, it is often determined indirectly, The most interesting exoplanets to study are certainly the tran- as only stars in binary systems can have their mass directly mea- siting exoplanets, as the transit light curve allows us to know sured if the system inclination is known. However, if an exo- the planetary radius. An additional radial velocity (RV) follow- planet is transiting its host star, the density of the star can be up provides the planetary mass and thus the planetary density. directly inferred from the transit light curve (Seager & Mallen-´ The three ingredients to estimate planetary bulk composition are Ornelas 2003). Then, in the case of bright stars, the radius can then gathered. But this is only true if the stellar radius and mass be directly determined using interferometry, which is a high an- 1 R. Ligi: Stellar and planetary properties of HD 219134. gular resolution technique aimed at measuring the angular diam- (Mourard et al. 2009; Ligi et al. 2013) is based on the CHARA eter of stars with a precision up to a few percent (Baines et al. array (ten Brummelaar et al. 2005), which takes advantage of 2010; Boyajian et al. 2012a,b; Huber et al. 2012; Creevey et al. the six 1 m telescopes distributed in a Y-shape to insure wide 2012; Ligi et al. 2012; Creevey et al. 2015; Ligi et al. 2016, (u,v) coverage. It can be used at medium (5000) or high spectral e.g.). The mass can thus be directly computed from the tran- resolution (30 000) and with baselines ranging from 34 to 331 sit and interferometric measurements. This method has recently m in the two telescope (2T), 3T, or 4T modes. The observations been used by Crida et al. (2018b,a) to derive the mass of the were calibrated following the sequence calibrator - science star very bright star 55 Cnc with a precision of 6.6% using the inter- - calibrator, and were performed using different configurations ferometric diameter measured by Ligi et al. (2016) and the den- (Table 1), mainly in the 2T mode at once to optimise the signal- sity from the transit light curve obtained for 55 Cnc e (Bourrier to-noise ratio (S/N) of the observations. The calibrator stars were et al. 2018). This yielded the best characterisation of the transit- selected into the SearchCal software1 (Table 2), and we used ing super-Earth 55 Cnc e so far and a new estimate of its internal the uniform disc diameter in the R band (UDDR) found in the composition. JSDC2 (Bourges´ et al. 2014) or SearchCal (Chelli et al. 2016) HD 219134 (HIP 114622, GJ 892) is also a bright (V=5.57) catalogue otherwise. However, for conservative reasons, we de- K3V star 6.5 parsecs away from us. Motalebi et al. (2015) first cided to use an uncertainty of 7% or that given in the JSDC1 detected four exoplanets around the star from RV measurements (Bonneau et al. 2006) if higher. We selected the calibrators with using the High Accuracy Radial velocity Planet Searcher for the several criteria: in the neighbourhood of the star, discarding vari- Northern hemisphere (HARPS-N) on the Telescopio Nazionale able stars and multiple systems, and with high squared visibili- Galileo (TNG). Moreover, Spitzer time-series photometric ob- ties, allowing an optimal measurement of the instrumental trans- servations allowed the detection of the transit of planet b, leading fer function. Finally, the data were reduced using the vegadrs to the estimate of a rocky composition. The same year, Vogt et al. pipeline (Mourard et al. 2009, 2011) developed at Observatoire (2015) claimed the detection of six planets around HD 219134 de la Coteˆ d’Azur. For each observation, we selected two non- from the analysis of RV obtained with the HIgh Resolution redundant spectral bands of 20 nm wide centred at 685 nm, 705 Echelle Spectrometer (HIRES) on Keck I Observatory and the nm, or 725 nm in most cases to derive the squared visibility (V2), Levy Spectrograph at the Automated Planet Finder Telescope but the reddest band is sometimes of bad quality or features ab- (Lick Observatory). These authors derived similar periods for sorption lines and cannot be used. In total, we collected 36 data planets b, c; and d, the other diverging because of the different points, which are shown in Fig. 1. Keplerian analysis of the RV signal leading to a different number of planets. Later, Gillon et al. (2017) reported additional Spitzer observations of the system that led to the discovery of the transit 2.2. Angular diameter of the second innermost planet, HD 219134 c. The two inner- The squared visibilities that we obtained (Fig. 1, coloured filled most planets seem rocky, but more interestingly, planet c shows circles) are well spread on the V2 curve. We note some disper- a higher density while it has a lower mass than planet b. The sion around 0:7 × 108=rad (corresponding to the E1E2 config- detailed planetary data and their relative differences place ad- uration) but it is taken into account in the computation of the ditional constraints on their interiors with implications to their error on the angular diameter. We also adopted a conservative formation and evolution. approach by setting a minimum error of 5% on V2 to balance the In this paper, we report new observations of HD 219134 us- known possible bias with VEGA (Mourard et al.